A Catalogue of Galactic Supernova Remnants
D.A.Green
Mullard Radio Astronomy Observatory
Cavendish Laboratory
Madingley Road
Cambridge CB3 0HE
UNITED KINGDOM
The sections of this document are:
Note: This page for quick local access. Links below are inactive. Select
entire catalog to get to all of Dave Green's links. (P. Slane 10/11/94)
This catalogue of Galactic supernova remnants (SNRs) is an updated version of
those presented in detail in Green (1984, 1988) and in summary form in Green
(1991) (hereafter Papers I, II, and III respectively). This version contains
182 SNRs (which is 8 more than in the summary catalogue of Paper III and 26
more than in the detailed catalogue of Paper II).
The catalogue is available as a summary listing of
the parameters for each remnant, and as detailed
listings (with references) for each object. Please also see for a
cross-reference list of other names used for these
SNRs, and the list of abbreviations used in the
detailed listings. A paper version of the full listings for all 182 remnants,
with the documentation, is available from me on request.
The summary listings will be included in the proceedings of IAU Colloquium 145
on `Supernovae and Supernova Remnants', held in Xian, China, 1993 May 22 to 29
(to be published by Cambridge University Press, eds. McCray, R. & Wang,
Z.). Please reference this paper for this version of the catalogue.
For each remnant in the catalogue the following parameters are given:
- `Galactic Coordinates' of the source centroid quoted to the nearest tenth
of a degree as is conventional.
- `Other Names' that are commonly used for the object. These are given in
parentheses if the remnant is only a part of the source.
- `Right Ascension' and `Declination' of the source centroid. The accuracy of
the quoted values depends on the size of the remnant; for small remnants they
are to the nearest few seconds of time and the nearest minute of arc
respectively, whereas for larger remnants they are rounded to coarser values,
but are in every case sufficient to specify a point within the boundary of the
remnant. These coordinates are deduced from radio maps rather than from X-ray
or optical observations, and are for B1950.0.
- `Angular Size' of the remnant, in arcminutes, usually taken from the
highest resolution radio map available, although for some barely resolved
sources that are thought to be SNRs the only available size is that from
Gaussian models after deconvolution with the observed beam size. The boundary
of most remnants approximates reasonably well to a circle or an ellipse; a
single value is quoted for the angular size of the more nearly circular
remnants, which is the diameter of a circle with an area equal to that of the
remnant, but for elongated remnants the product of two values is quoted, and
these are the major and minor axes of the remnant boundary modelled as an
ellipse. In a few cases an ellipse is not a satisfactory description of the
boundary of the object (refer to the description of the individual object given
in its catalogue entry), although an angular size is still quoted for
information. For `filled-centre' remnants the size quoted is for the largest
extent of the observed radio emission, not, as at times has been used, the
half-width of the centrally brightened peak.
- `Flux Density' of the remnant at 1 GHz in jansky. This is not a measured
value, but that deduced from the observed radio frequency spectrum of the
source. The frequency of 1 GHz is chosen because flux density measurements at
frequencies both above and below this value are usually available.
- `Spectral Index' of the integrated radio emission from the remnant, either
a value that is quoted in the literature, or one deduced from the available
integrated flux densities of the remnant. For several SNRs a simple spectral
model is not adequate to describe their radio emission because there is
evidence that the spectral index varies across the face of the remnant or that
the integrated spectrum is curved, and in these cases the spectral index is
given as `varies' (refer to the description of the remnant and recent
references in the catalogue entry for more information). In a few cases, where
the remnant is highly confused with thermal emission, the spectral index is
given as `?' since no value can be deduced with any confidence.
- `Type' of the SNR, either `S', `F' or `C' if the remnant shows a `shell',
`filled-centre' or `composite' (or `combination') radio structure (or `S?',
`F?' or `C?', respectively, if there is some uncertainty), or `?' in several
cases where an object is conventionally regarded as an SNR even though its
nature is poorly known or not well understood.
The following objects, which were listed in the catalogue in Paper I, have been
removed from the catalogue because they are no longer thought to be remnants,
or are poorly observed (see Paper II for references and further details):
G2.4+1.4, G41.9-4.1 (=CTB 73, PKS 1920+06), G47.6+6.1 (=CTB 63), G53.9+0.3
(part of HC40), G93.4+1.8 (=NRAO 655), G123.2+2.9, G194.7+0.4 (the Origem
Loop), G287.8-0.5, G322.3-1.2 (=Kes 24) and G343.0-6.0.
G350.1-0.3, which was listed in the catalogue in Paper II, was removed as it is
no longer thought to be a SNR (see Paper III for details). No objects listed in
the catalogue in Paper III have since been removed.
The following objects, which have been reported as SNRs, but have not been
included in any of SNR catalogues, have subsequently been shown not to be SNRs:
- G70.7+1.2 which was reported as a SNR by Reich et al. (1985), but this has
not been confirmed by subsequent observations (see Green 1986; de Muizon et al.
1988; Becker & Fesen 1988; Caswell 1988; Bally et al. 1989).
- G81.6+1.0 a possible SNR in W75 reported by Ward-Thompson & Robson
(1991) is instead a thermal source, because of its thermal radio spectrum, and
high infrared-to-radio emission (see the observations in Wendker, Higgs &
Landecker 1991).
- Green & Gull (1984) suggested that G227.1+1.0 as a very young SNR, but
subsequent observations (Channan et al. 1986; Green & Gull 1986) have shown
that this is most likely an extragalactic source, not an SNR.
- A candidate SNR, G274.7-2.8, identified by Helfand & Channan (1989), has
been shown not to be a SNR by Caswell & Stewart (1991).
- G25.5+0.2, which was reported as a very young SNR by Cowan et al. (1990),
although this identification was not certain (see White & Becker 1990;
Green 1990; Zijlstra 1991). Sramek et al. (1992) report the detection of
recombination lines from this source.
- Most of the possible SNRs listed by Gorham (1990) have been shown not to
be SNRs by Gorham, Kulkarni & Prince (1993).
Some entries in the catalogue have been renamed, due to improved observations
revealing a larger true extent for the object (G5.3-1.0 is now G5.4-1.2;
G193.3-1.5 is now G192.8-1.1; G308.7+0.0 is now G308.8-0.1).
The following new remnants were added to the catalogue of Paper II: G0.9+0.1,
G1.9+0.3, G5.9+3.1, G6.4+4.0, G8.7-0.1, G16.8-1.1, G18.9-1.1, G20.0-0.2,
G27.8+0.6, G30.7+1.0, G31.5-0.6, G36.6-0.7, G42.8+0.6, G45.7-0.4, G54.1+0.3,
G73.9+0.9, G179.0+2.6, G312.4-0.4, G357.7+0.3 and G359.1-0.9.
The following new remnants were added to the catalogue of Paper III: G4.2-3.5,
G5.2-2.6, G6.1+1.2, G8.7-5.0, G13.5+0.2, G15.1-1.6, G16.7+0.1, G17.4-2.3,
G17.8-2.6, G30.7-2.0, G36.6+2.6, G43.9+1.6, G59.8+1.2, G65.1+0.6, G68.6-1.2,
G69.7+1.0, G279.0+1.1, G284.3-1.8 (=MSH 10-5(3)), G358.4-1.9 and G359.0-0.9.
Since Paper III, the following SNRs have been added to the catalogue:
- Three new remnants (G59.5+0.1, G67.7+1.8 and G84.9+0.5) of the the eleven
possible SNRs reported by Taylor, Wallace & Goss (1992).
- G156.2+5.7, which was first identified from X-ray observations by ROSAT
(Pfeffermann, Aschenbach & Predehl 1991).
- G318.9+0.4, a complex of radio arcs reported by Whiteoak (1990).
- G322.5-0.1, reported by Whiteoak (1992).
- G343.1-2.3, an incomplete radio shell, with an associated pulsar (McAdam,
Osborne & Parkinson 1993).
- G348.5-0.0, a radio arc near G348.5+0.1 (=CTB 37A), revealed by Kassim,
Baum & Weiler (1991).
The following are possible SNRs for which further observations are required to
confirm their nature.
- Eight possible remnants (G45.9-0.1, G55.2+0.5, G63.7+1.1, G71.6-0.5,
G72.2-0.3, G76.9+0.9, G83.0-0.2 and G85.2-1.2) of the the eleven reported by
Taylor, Wallace & Goss (1992).
- G287.6-0.6 and G343.0-6.0 --- both of which were listed in Paper I as SNRs
but have been removed from the catalogue because only limited observations are
available --- should be considered as possible SNRs (see Tateyama, Strauss &
Kaufmann 1991 for G287.6-0.6).
- G284.2-1.8 (=MSH 10-5(3)), which was listed in early SNR catalogues, but
subsequently rejected because of its apparent thermal spectrum (see Paper II
for details). Ruiz & May (1986) report optical and CO radio observations that
indicate the presence of shock-excited material, supporting the SNR
identification, although the parameters of any SNR are not well defined.
- A possible SNR within the Puppis A remnant (Winkler et al. 1989).
- G300.1+9.4, a possible SNR reported by Dubner, Colomb & Giacani (1986).
- G203.2-12.3, a filamentary optical ring identified as a SNR by Winkler
& Reipurth (1992).
- G315.8-0.0, a possible `shell' SNR with a remarkable collimated `jet' of
radio emission, reported by Kesteven et al. (1987), although this source has an
unusually steep spectrum.
- A possible SNR near l=32d reported by Thompson, Djorgovski &
Decarvalho (1991).
- A faint, poorly defined possible remnant G41.1+1.2 reported by Gorham,
Kulkarni & Prince et al. (1993).
- A possible large SNR in Lupus near l=347d, b=22d (Reigler, Agrawal &
Gull 1980; Colomb, Dubner & Giacani 1984).
- G1.0-0.1, a possible SNR near the Galactic centre reported by Downes et
al. (1978).
- G75.5+2.4, a possible old SNR in Cygnus (Nichols-Bohlin & Fesen 1993).
Other possible SNRs are reported by Ho et al. (1985), Gosachinskii (1985),
Odegard (1986), Fürst, Reich & Sofue (1987), Routledge & Vaneldik
(1988), Kassim (1988), Helfand et al. (1989), Meaburn et al. (1991), Leahy,
Nousek & Garmire (1992), and Dubner et al. (1992).
Finally, it should be noted that some radio loops in the Galactic plane (see
Berkhuijsen 1973) may be parts of very large, old SNRs, but they have not been
included in the catalogue.
As noted in Paper II, the following sources are listed in the catalogue as
SNRs, although, as discussed in each case, the identifications are not certain:
G5.4-1.2, G39.7-2.0 (=W50), G65.7+1.2 (=DA 495), G69.0+2.7 (=CTB 80),
G357.7-0.1. The nature of G318.9+0.4 is also uncertain (see Whiteoak 1990).
There are also many objects that have been identified as SNRs and are listed in
the catalogue, although they have been barely resolved in the available
observations, or are faint, and have not been well separated from confusing
background or nearby thermal emission, and their identification as SNRs, or at
least their parameters remain uncertain (see Paper II).
The detailed catalogue includes, for each remnant,
notes on a variety of topics. First, it is noted if other Galactic coordinates
have at times been used to label it (usually before good observations have
revealed the full extent of the object), if the SNR is thought to be the
remnant of a historical SN, or if the nature of the source as an SNR has been
questioned (in which case an appropriate reference is usually given later in
the entry). Brief descriptions of the remnant from the available radio, optical
and X-ray observations as applicable are then given, together with notes on
available distance determinations, and any point sources or pulsars in the
field of the object (although they may not necessarily be related to the
remnant). Finally, appropriate references are given for each remnant, complete
with journal, volume, page, and a short description of what information each
paper contains (for radio observations these include the telescopes used, the
observing frequencies and resolutions, together with any flux density
determinations). These references are not complete, but cover representative
and recent observations of the remnant, and they should themselves include
references to earlier work. This version of the catalogue contains nearly two
hundred more references in the detailed listings than in Paper II. The
references do not generally include large observational surveys --- of
particular interest in this respect are: the Effelsberg 100-m survey at 2.7 GHz
of the Galactic plane 358d < l < 240d, |b| < 5d by Reich et al. (1990) and
Fürst et al. (1990); the review of Einstein X-ray imaging and FPCS
observations of Galactic SNRs by Seward (1990) and Lum et al. (1992)
respectively; the survey of IRAS observations of SNRs and their immediate
surroundings by Arendt (1989) and by Saken, Fesen & Shull (1992); and the
survey of HI emission towards SNRs by Koo & Heiles (1991).
- Arendt, R.G., 1989. ApJS, 70, 181.
- Bally, J., Pound, M.W., Stark, A.A., Israel, F., Hirano, N., Kameya, O.,
Sunada, K., Hayashi, M., Thronson, H. Jr & Hereld, M., 1989. ApJ, 338,
L65.
- Becker, R.H. & Fesen, R.A., 1988. ApJ, 334, L40.
- Berkhuijsen, E.M., 1973. AA, 24, 143.
- Caswell, J.L., 1988. In SNRISM, p269.
- Caswell, J.L. & Stewart, R.T., 1991. PASA, 9, 103.
- Caswell, J.L. Kesteven, M.J., Stewart, R.T., Milne, D.K. & Haynes,
R.F., 1992. ApJ, 399, L151.
- Channan, G.A., Helfand, D.J., Spinrad, H. & Ebneter, K., 1986. Nature,
320, 41.
- Colomb, F.R., Dubner, G.M. & Giacani, E.B., 1984. AA, 130, 294.
- Cowan, J.J., Ekers, R.D., Goss, W.M., Sramek, R.A., Roberts, D.A. &
Branch, D., 1989. MN, 241, 613.
- de Muizon, M., Strom, R.G., Oort, M.J.A., Claas, J.J. & Braun, R.,
1988. AA, 193, 248.
- Downes, D., Goss, W.M., Schwarz, U.J. & Wouterloot, J.G.A., 1978. AAS,
35, 1.
- Dubner, G.M., Colomb, F.R. & Giacani, E.B., 1986. ApJ, 91, 343.
- Dubner, G., Giacani, E., Cappa de Nicolau, C., & Regnoso, E., 1992.
AAS, 96, 505.
- Fürst, E., Reich, W. & SoFü, Y., 1987. AAS, 71, 63.
- Fürst, E., Reich, W., Reich, P. & Reif, K., 1990, AAS, 85,
691.
- Gorham, P.W., 1990. ApJ, 364, 187.
- Gorham, P.W., Kulkarni, S.K. & Prince, T.A., 1993. AJ, 105, 314.
- Gosachinskii, I.V., 1985. SA, 29, 128.
- Green, D.A., 1984. MN, 209, 449 (Paper I).
- Green, D.A., 1986. MN, 219, 39P.
- Green, D.A., 1988. ASS, 148, 3 (Paper II).
- Green, D.A., 1990. AJ, 100, 1241.
- Green, D.A., 1991. PASP, 103, 209 (Paper III).
- Green, D.A. & Gull, S.F., 1984. Nature, 312, 527.
- Green, D.A. & Gull, S.F., 1986. Nature, 320, 42.
- Helfand, D.J. & Channan, G.A., 1989. AJ, 98, 1652.
- Helfand, D., Velusamy, T., Becker, R.H. & Lockman, F.J., 1989. ApJ,
341, 151.
- Ho, P.T., Jackson, J.M., Barrett, A.H. & Armstrong, J.T., 1985. ApJ,
288, 575.
- Kassim, N.E., 1988. ApJ, 328, L55.
- Kassim, N., Baum, S.A. & Weiler, K.W., 1991. ApJ, 374, 212.
- Kesteven, M.J., Caswell, J.L, Roger, R.S., Milne, D.K., Haynes, R.F. &
- Wellington, K.J., 1987. AJP, 40, 855.
- Koo, B.-C. & Heiles, C., 1991. ApJ, 382, 204.
- Leahy, D.A., Nousek, J. & Garmire, G., 1992, ApJ, 385, 561.
- Lum, K.S.K., Canizares, C.R., Clark, S.W., Coyne, J.M., Markert, T.H.,
Saez,
- P.J., Schattenburg, M.L. & Winkler, P.F., 1992, ApJS, 78, 423.
- McAdam, W.B., Osborne, J.L. & Parkinson, M.L., 1993. Nature, 361,
516.
- Meaburn, J., Goudis, C., Solomos, N. & Laspias, I., 1991. AA, 252,
291.
- Nichols-Bohlin, J. & Fesen, R.A., 1993. AJ, 105, 672.
- Odegard, N., 1986. AJ, 92, 1372.
- Pfeffermann, E., Aschenbach, B. & Predehl, P., 1991. AA, 246, L28.
- Reich, W., Fürst, E., Altenhoff, W.J., Reich, P. & Junkes, N.,
1985. AA, 151, L10.
- Reich, W., Fürst, E., Reich, P. & Reif, K., 1990, AAS, 85,
633.
- Reigler, G.R., Agrawal, P.C. & Gull, S.F., 1988. ApJ, 235, L71.
- Routledge, D. & Vaneldik, J.F., 1988. ApJ, 326, 751.
- Ruiz, M.T. & May, J., 1987. ApJ, 309, 667.
- Saken, J.M., Fesen, R.A. & Shull, J.M., 1992. ApJS, 81, 715.
- Seward, F.D., 1990. ApJS, 73, 781.
- Sramek, R.A., Cowan, J.J., Roberts, D.A., Goss, W.M. & Ekers, R.D.,
1992. AJ, 104, 705.
- Tateyama, C.E., Strauss, F.M. & Kaufmann, P., 1991. MN, 249, 716.
- Taylor, A.R., Wallace, B.J. & Goss, W.M., 1992. AJ, 103, 931.
- Thompson, D.J., Djorgovski, S. & Decarvalho, R.R., 1991. PASP, 102,
487.
- Ward-Thompson, D. & Robson, 1991. MN, 248, 670.
- Wendker, H.I., Higgs, L.A. & Landecker, T.L., 1991. AA, 241, 551.
- White, R.L. & Becker, R.H., 1990. MN, 244, 12P.
- Whiteoak, J.B.Z., 1990. Nature, 347, 157.
- Whiteoak, J.B.Z., 1992. MN, 256, 121.
- Winkler, P.F. & Reipurth, B., 1992. ApJ, 389, L25.
- Winkler, P.F., Kirshner, R.P., Hughes, J.P. & Heathcote, S.R. 1989.
Nature, 337, 48.
- Zijlstra, A.A., 1991. MN, 248, 11P.
Please e-mail me, or use this form, if you have
any comments. In particular, I'd like to know of references for any objects
that have been described as SNRs, but that are no longer thought to be
remnants, or for possible SNRs not listed in the catalogue that are not already
discussed in Section 2.1 or Section 2.3
respectively.
Dave Green/MRAO, Cambridge, UK/D.A.Green@MRAO.CAM.AC.UK